A multiwavelength investigation of the massive eclipsing binary Cygnus OB2 #5

Linder, N.; Rauw, Grégor; Manfroid, Jean; Damerdji, Y.; Becker, M. De; Royer, P.; Vreux, Jean-Marie

doi:10.1051/0004-6361:200810974

Cited by 39 publications

(102 citation statements)

References 48 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Hanson 2003;Torres-Dodgen et al 1991;and Kiminki et al 2007). Therefore they do not agree with the distance estimate of 900-950 pc obtained by Linder et al (2009) from the light curve modelling of Cyg OB2 #5. A distance of 900 pc would imply radii that are ∼half those currently derived from the modelling.…”

Section: Light and Radial Velocity Curve Analysiscontrasting

confidence: 68%

“…We note that a system composed of O7 Iaf & O9 Iaf stars is also compatible with the other massive evolved binaries in Cyg OB2. Indeed, the 6.6 day Ofpe/WNL+O6.5-7 binary Cyg OB2 #5 (Linder et al 2009) appears to be remarkably similar to B17, although with the Ofpe/WNL star being slightly more evolved than the O9 Iaf secondary in B17. The slightly longer period of Cyg OB2 #5 can be explained by one or more from (i) initial birth parameters, (ii) mass transfer from one star to the other and (iii) mass lost by both stars via stellar winds.…”

Section: Discussionmentioning

confidence: 88%

See 1 more Smart Citation

The eclipsing, double-lined, Of supergiant binary Cygnus OB2-B17

Stroud

Clark

Negueruela

et al. 2010

A&A

View full text Add to dashboard Cite

Context. Massive, eclipsing, double-lined, spectroscopic binaries are not common but are necessary to understand the evolution of massive stars as they are the only direct way to determine stellar masses. They are also the progenitors of energetic phenomena such as X-ray binaries and γ-ray bursts.Aims. We present a photometric and spectroscopic analysis of the candidate binary system Cyg OB2-B17 to show that it is indeed a massive evolved binary. Methods. We utilise V band and white-light photometry to obtain a light curve and period of the system, and spectra at different resolutions to calculate preliminary orbital parameters and spectral classes for the components. Results. Our results suggest that B17 is an eclipsing, double-lined, spectroscopic binary with a period of 4.0217 ± 0.0004 days, with two massive evolved components with preliminary classifications of O7 and O9 supergiants. The radial velocity and light curves are consistent with a massive binary containing components with similar luminosities, and in turn with the preliminary spectral types and age of the association.

show abstract

Section: Light and Radial Velocity Curve Analysiscontrasting

confidence: 68%

Section: Discussionmentioning

confidence: 88%

The eclipsing, double-lined, Of supergiant binary Cygnus OB2-B17

Stroud

Clark

Negueruela

et al. 2010

A&A

View full text Add to dashboard Cite

show abstract

“…To check our results, we looked at the other sources in the Swift field-of-view. Cyg OB2 #5 and 12 are known to vary, but unfortunately, their variations are not fully explained and predictable (Linder et al 2009;Rauw 2011). The behavior of the collidingwind binary Cyg OB2 #8A is, however, well known (De Becker et al 2006;Blomme et al 2010), and the Swift data are here fully consistent with the XMM-Newton and ASCA data, when taking the errors due to a lower number of counts in the Swift data into account.…”

Section: The Spectrasupporting

confidence: 53%

The 2.35 year itch of Cygnus OB2 #9

Nazé

Mahy

Damerdji

et al. 2012

A&A

Self Cite

View full text Add to dashboard Cite

Context. Nonthermal radio emission in massive stars is expected to arise in wind-wind collisions occurring inside a binary system. One such case, the O-type star Cyg OB2 #9, was proven to be a binary only four years ago, but the orbital parameters remained uncertain. The periastron passage of 2011 was the first one to be observable under good conditions since the discovery of binarity. Aims. In this context, we have organized a large monitoring campaign to refine the orbital solution and to study the wind-wind collision.Methods. This paper presents the analysis of optical spectroscopic data, as well as of a dedicated X-ray monitoring performed with Swift and XMM-Newton. Results. In light of our refined orbital solution, Cyg OB2 #9 appears as a massive O+O binary with a long period and high eccentricity; its components (O5-5.5I for the primary and O3-4III for the secondary) have similar masses and similar luminosities. The new data also provide the first evidence that a wind-wind collision is present in the system. In the optical domain, the broad Hα line varies, displaying enhanced absorption and emission components at periastron. X-ray observations yield the unambiguous signature of an adiabatic collision, because as the stars approach periastron, the X-ray luminosity closely follows the 1/D variation expected in that case. The X-ray spectrum appears, however, slightly softer at periastron, which is probably related to winds colliding at slightly lower speeds at that time. Conclusions. It is the first time that such a variation has been detected in O+O systems, and the first case where the wind-wind collision is found to remain adiabatic even at periastron passage.

show abstract

“…The best-fit model has an inclination i = 62 • and provides a close match to the light curve from φ ∼ 0.5 to φ ∼ 1, although the region around φ = 0.2−0.4 is less well reproduced. Although the nightfall code supports additional features such as "hot spots" that may provide a better fit to this portion of the light curve (see, for example, the model of Cyg OB2#5 presented by Linder et al 2009), we consider further refinement of the model inappropriate given the limitations of the photometric dataset used. Parameters derived from the light curve model are listed in Table 2, although we stress that our primary goal is to constrain the inclination of the system and other parameters should be regarded as provisional pending acquisition of longer-term photometry.…”

Section: Light Curvementioning

confidence: 99%

A VLT/FLAMES survey for massive binaries in Westerlund 1

Ritchie¹,

Clark²,

Negueruela³

et al. 2010

A&A

View full text Add to dashboard Cite

Context. Westerlund 1 is a young, massive Galactic starburst cluster that contains a rich coeval population of Wolf-Rayet stars, hotand cool-phase transitional supergiants, and a magnetar. Aims. We use spectroscopic and photometric observations of the eclipsing double-lined binary W13 to derive dynamical masses for the two components, in order to determine limits for the progenitor masses of the magnetar CXOU J164710.2-455216 and the population of evolved stars in Wd1. Methods. We use eleven epochs of high-resolution VLT/FLAMES spectroscopy to construct a radial velocity curve for W13. R-band photometry is used to constrain the inclination of the system. Results. W13 has an orbital period of 9.2709 ± 0.0015 days and near-contact configuration. The shallow photometric eclipse rules out an inclination greater than 65 • , leading to lower limits for the masses of the emission-line optical primary and supergiant optical secondary of 21.4 ± 2.6 M and 32.8 ± 4.0 M respectively, rising to 23.2 +3.3 −3.0 M and 35.4 +5.0 −4.6 M for our best-fit inclination 62 +3 −4 degrees. Comparison with theoretical models of Wolf-Rayet binary evolution suggest the emission-line object had an initial mass in excess of ∼35 M , with the most likely model featuring highly non-conservative late-Case A/Case B mass transfer and an initial mass in excess of 40 M . Conclusions. This result confirms the high progenitor mass of the magnetar CXOU J164710.2-455216 inferred from its membership in Wd1, and represents the first dynamical constraint on the progenitor mass of any magnetar. The red supergiants in Wd1 must have similar progenitor masses to W13 and are therefore amongst the most massive stars to undergo a red supergiant phase, representing a challenge for population models that suggest stars in this mass range end their redwards evolution as yellow hypergiants.

show abstract

A multiwavelength investigation of the massive eclipsing binary Cygnus OB2 #5

Cited by 39 publications

References 48 publications

The eclipsing, double-lined, Of supergiant binary Cygnus OB2-B17

The eclipsing, double-lined, Of supergiant binary Cygnus OB2-B17

The 2.35 year itch of Cygnus OB2 #9

A VLT/FLAMES survey for massive binaries in Westerlund 1

Contact Info

Product

Resources

About